Manuela Campanelli (scientist)

Last updated

Manuela Campanelli
Born
Switzerland
Alma mater
Occupation(s)astrophysicist, professor
Known forNumerical Relativity:

Binary Black Holes and Gravitational Waves. GravitoMagnetohydrodynamics: Black Hole Accretion

Compact Binary Mergers and Gravitational Core Collapse

Contents

Manuela Campanelli is a distinguished professor of astrophysics of the Rochester Institute of Technology. [1] She also holds the John Vouros endowed professorship at RIT and is the director of its Center for Computational Relativity and Gravitation. [2] [3] Her work focuses on the astrophysics of merging black holes and neutron stars, which are powerful sources of gravitational waves, electromagnetic radiation and relativistic jets. This research is central to the fields of relativistic astrophysics and gravitational-wave astronomy.

She is a Fellow of the American Physical Society (2009), [4] a Fellow of International Society on General Relativity and Gravitation Fellowship (2019), [5] and a recipient of the Richard A. Isaacson award in Gravitational-Wave Science of the APS (2024). [6]

Professional work

Campanelli is known for her groundbreaking work in gravitational wave astrophysics. She was lead author on a paper that produced a breakthrough in gravitational wave astrophysics [7] in 2005; she also discovered that supermassive black holes can be ejected from their host galaxies at up to 4000 km/s. [8] She then moved on to studying the behavior of matter around inspiraling black holes, both in the mini disks size, [9] growth [10] and potential electromagnetic emissions. [11] She has received many awards, including the Marie Curie Fellowship (1998), [12] the RIT Trustees Scholarship Award, [13] was mentioned in Kip Thorne's Nobel Prize lecture [14] [15] and her paper for the gravitational wave breakthrough was listed as one of the landmark papers of the century by the American Physical Society. [16] She was also the chair of the APS topical group in gravitation in 2013. [17]

Biography

Campanelli was born in Switzerland, but moved with her family to Italy at the age of 14. She received an undergraduate degree in applied mathematics from the University of Perugia in Italy in 1991, and a PhD in theoretical physics from the University of Bern in Switzerland in 1996. She moved then to the University of Utah and then to the Max Planck Institute in Germany, where she began to use supercomputer simulations to understand how black holes coalesce. [18]

After five years at the University of Texas at Brownsville, [18] Dr. Campanelli joined the Rochester Institute of Technology in 2007. [19]

Publications

Books

Journal articles

Related Research Articles

<span class="mw-page-title-main">General relativity</span> Theory of gravitation as curved spacetime

General relativity, also known as the general theory of relativity, and as Einstein's theory of gravity, is the geometric theory of gravitation published by Albert Einstein in 1915 and is the current description of gravitation in modern physics. General relativity generalizes special relativity and refines Newton's law of universal gravitation, providing a unified description of gravity as a geometric property of space and time or four-dimensional spacetime. In particular, the curvature of spacetime is directly related to the energy and momentum of whatever matter and radiation are present. The relation is specified by the Einstein field equations, a system of second-order partial differential equations.

In general relativity, a naked singularity is a hypothetical gravitational singularity without an event horizon.

<span class="mw-page-title-main">Quantum gravity</span> Description of gravity using discrete values

Quantum gravity (QG) is a field of theoretical physics that seeks to describe gravity according to the principles of quantum mechanics. It deals with environments in which neither gravitational nor quantum effects can be ignored, such as in the vicinity of black holes or similar compact astrophysical objects, such as neutron stars, as well as in the early stages of the universe moments after the Big Bang.

<span class="mw-page-title-main">Timeline of gravitational physics and relativity</span>

The following is a timeline of gravitational physics and general relativity.

The no-hair theorem states that all stationary black hole solutions of the Einstein–Maxwell equations of gravitation and electromagnetism in general relativity can be completely characterized by only three independent externally observable classical parameters: mass, electric charge, and angular momentum. Other characteristics are uniquely determined by these three parameters, and all other information about the matter that formed a black hole or is falling into it "disappears" behind the black-hole event horizon and is therefore permanently inaccessible to external observers after the black hole "settles down". Physicist John Archibald Wheeler expressed this idea with the phrase "black holes have no hair", which was the origin of the name.

Tests of general relativity serve to establish observational evidence for the theory of general relativity. The first three tests, proposed by Albert Einstein in 1915, concerned the "anomalous" precession of the perihelion of Mercury, the bending of light in gravitational fields, and the gravitational redshift. The precession of Mercury was already known; experiments showing light bending in accordance with the predictions of general relativity were performed in 1919, with increasingly precise measurements made in subsequent tests; and scientists claimed to have measured the gravitational redshift in 1925, although measurements sensitive enough to actually confirm the theory were not made until 1954. A more accurate program starting in 1959 tested general relativity in the weak gravitational field limit, severely limiting possible deviations from the theory.

Numerical relativity is one of the branches of general relativity that uses numerical methods and algorithms to solve and analyze problems. To this end, supercomputers are often employed to study black holes, gravitational waves, neutron stars and many other phenomena described by Albert Einstein's theory of general relativity. A currently active field of research in numerical relativity is the simulation of relativistic binaries and their associated gravitational waves.

In general relativity, a geon is a nonsingular electromagnetic or gravitational wave which is held together in a confined region by the gravitational attraction of its own field energy. They were first investigated theoretically in 1955 by J. A. Wheeler, who coined the term as a contraction of "gravitational electromagnetic entity".

A ring singularity or ringularity is the gravitational singularity of a rotating black hole, or a Kerr black hole, that is shaped like a ring.

Analog models of gravity are attempts to model various phenomena of general relativity using other physical systems such as acoustics in a moving fluid, superfluid helium, or Bose–Einstein condensate; gravity waves in water; and propagation of electromagnetic waves in a dielectric medium. These analogs serve to provide new ways of looking at problems, permit ideas from other realms of science to be applied, and may create opportunities for practical experiments within the analog that can be applied back to the source phenomena.

<span class="mw-page-title-main">Gravitational-wave astronomy</span> Branch of astronomy using gravitational waves

Gravitational-wave astronomy is a subfield of astronomy concerned with the detection and study of gravitational waves emitted by astrophysical sources.

<span class="mw-page-title-main">Relativistic images</span> Images of gravitational lensing

Relativistic images are images of gravitational lensing which result due to light deflections by angles .

<span class="mw-page-title-main">Binary black hole</span> System consisting of two black holes in close orbit around each other

A binary black hole (BBH), or black hole binary, is a system consisting of two black holes in close orbit around each other. Like black holes themselves, binary black holes are often divided into binary stellar black holes, formed either as remnants of high-mass binary star systems or by dynamic processes and mutual capture; and binary supermassive black holes, believed to be a result of galactic mergers.

In astrophysics, the chirp mass of a compact binary system determines the leading-order orbital evolution of the system as a result of energy loss from emitting gravitational waves. Because the gravitational wave frequency is determined by orbital frequency, the chirp mass also determines the frequency evolution of the gravitational wave signal emitted during a binary's inspiral phase. In gravitational wave data analysis, it is easier to measure the chirp mass than the two component masses alone.

<span class="mw-page-title-main">Extreme mass ratio inspiral</span>

In astrophysics, an extreme mass ratio inspiral (EMRI) is the orbit of a relatively light object around a much heavier object, that gradually spirals in due to the emission of gravitational waves. Such systems are likely to be found in the centers of galaxies, where stellar mass compact objects, such as stellar black holes and neutron stars, may be found orbiting a supermassive black hole. In the case of a black hole in orbit around another black hole this is an extreme mass ratio binary black hole. The term EMRI is sometimes used as a shorthand to denote the emitted gravitational waveform as well as the orbit itself.

<span class="mw-page-title-main">First observation of gravitational waves</span> Detection made by LIGO and Virgo interferometers (2015)

The first direct observation of gravitational waves was made on 14 September 2015 and was announced by the LIGO and Virgo collaborations on 11 February 2016. Previously, gravitational waves had been inferred only indirectly, via their effect on the timing of pulsars in binary star systems. The waveform, detected by both LIGO observatories, matched the predictions of general relativity for a gravitational wave emanating from the inward spiral and merger of a pair of black holes of around 36 and 29 solar masses and the subsequent "ringdown" of the single resulting black hole. The signal was named GW150914. It was also the first observation of a binary black hole merger, demonstrating both the existence of binary stellar-mass black hole systems and the fact that such mergers could occur within the current age of the universe.

<span class="mw-page-title-main">Carlos Lousto</span>

Carlos O. Lousto is a Distinguished Professor in the School of Mathematical Sciences in Rochester Institute of Technology, known for his work on black hole collisions.

In gravitational wave astronomy, a golden binary is a binary black hole collision event whose inspiral and ringdown phases have been measured accurately enough to provide separate measurements of the initial and final black hole masses.

<span class="mw-page-title-main">Frans Pretorius</span>

Frans Pretorius is a South African and Canadian physicist, specializing in computer simulations in astrophysics and numerical solutions of Einstein's field equations. He is professor of physics at Princeton University and director of the Princeton Gravity Initiative.

Ground-based interferometric gravitational-wave search refers to the use of extremely large interferometers built on the ground to passively detect gravitational wave events from throughout the cosmos. Most recorded gravitational wave observations have been made using this technique; the first detection, revealing the merger of two black holes, was made in 2015 by the LIGO sites.

References

  1. ↑ "Manuela Campanelli". rit.edu. Rochester Institute of Technology . Retrieved 10 August 2016.
  2. ↑ "Welcome | Center for Computational Relativity and Gravitation (CCRG)". ccrg.rit.edu. Retrieved 22 May 2024.
  3. ↑ "New Wave Astronomy". rit.edu. Rochester Institute of Technology. Retrieved 10 August 2016.
  4. ↑ "APS Fellow Archive".
  5. ↑ "Fellows". The International Society on General Relativity & Gravitation. Retrieved 22 May 2024.
  6. ↑ "Richard A. Isaacson Award in Gravitational-Wave Science". www.aps.org. Retrieved 22 May 2024.
  7. ↑ Campanelli, M.; Lousto, C. O.; Marronetti, P.; Zlochower, Y. (22 March 2006). "Accurate Evolutions of Orbiting Black-Hole Binaries without Excision". Physical Review Letters. 96 (11): 111101. arXiv: gr-qc/0511048 . Bibcode:2006PhRvL..96k1101C. doi:10.1103/PhysRevLett.96.111101. PMID   16605808. S2CID   5954627.
  8. ↑ Campanelli, Manuela; Lousto, Carlos O.; Zlochower, Yosef; Merritt, David (7 June 2007). "Maximum Gravitational Recoil". Physical Review Letters. 98 (23): 231102. arXiv: gr-qc/0702133 . Bibcode:2007PhRvL..98w1102C. doi:10.1103/PhysRevLett.98.231102. PMID   17677894. S2CID   29246347.
  9. ↑ Bowen, Dennis B.; Mewes, Vassilios; Campanelli, Manuela; Noble, Scott C.; Krolik, Julian H.; Zilhão, Miguel (24 January 2018). "Quasi-periodic Behavior of Mini-disks in Binary Black Holes Approaching Merger". The Astrophysical Journal. 853 (1): L17. arXiv: 1712.05451 . Bibcode:2018ApJ...853L..17B. doi: 10.3847/2041-8213/aaa756 . ISSN   2041-8213. S2CID   118926956.
  10. ↑ Noble, Scott C.; Mundim, Bruno C.; Nakano, Hiroyuki; Krolik, Julian H.; Campanelli, Manuela; Yosef Zlochower; Yunes, Nicolás (2012). "Circumbinary Magnetohydrodynamic Accretion into Inspiraling Binary Black Holes". The Astrophysical Journal. 755 (1): 51. arXiv: 1204.1073 . Bibcode:2012ApJ...755...51N. doi:10.1088/0004-637X/755/1/51. ISSN   0004-637X. S2CID   17805470.
  11. ↑ d’Ascoli, Stéphane; Noble, Scott C.; Bowen, Dennis B.; Campanelli, Manuela; Krolik, Julian H.; Mewes, Vassilios (2 October 2018). "Electromagnetic Emission from Supermassive Binary Black Holes Approaching Merger". The Astrophysical Journal. 865 (2): 140. arXiv: 1806.05697 . Bibcode:2018ApJ...865..140D. doi: 10.3847/1538-4357/aad8b4 . ISSN   1538-4357. S2CID   119243049.
  12. ↑ "Center for Computational Relativity and Gravitation (CCRG)". ccrg.rit.edu. Retrieved 23 December 2018.
  13. ↑ "Trustees Scholarship Award | RIT Faculty Awards". www.rit.edu. Retrieved 23 December 2018.
  14. ↑ Nobel Prize, Nobel Lecture: Kip Thorne, Nobel Prize in Physics 2017 , retrieved 23 December 2018
  15. ↑ Thorne, Kip S. (2019). "LIGO and Gravitational Waves, III: Nobel Lecture, December 8, 2017". Annalen der Physik. 531 (1). Bibcode:2019AnP...53100350T. doi: 10.1002/andp.201800350 . S2CID   125787651.
  16. ↑ "2015 - General Relativity's Centennial". Physical Review Journals. 18 September 2015. Retrieved 23 December 2018.
  17. ↑ "Past Executive Committees". www.aps.org. Retrieved 23 December 2018.
  18. 1 2 "Manuela Campanelli". Physics Central. American Physical Society . Retrieved 10 August 2016.
  19. ↑ "Trustees Scholarship Award". rit.edu. Rochester Institute of Technology. Retrieved 10 August 2016.
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